Coronal radiation of a cusp of spun-up stars and the X-ray luminosity of Sgr A*

Details Coronal radiation of a cusp of spun-up stars and the X-ray luminosity of Sgr A* Coronal radiation of a cusp of spun-up stars and the X-ray luminosity of Sgr A*

2011-08-13

arxiv.org/abs/1108.2778v2

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

18 pages, 7 figures. Accepted to MNRAS

Scientific paper

Chandra has detected optically thin, thermal X-ray emission with a size of ~1 arcsec and luminosity ~10^33 erg/s from the direction of the Galactic supermassive black hole (SMBH), Sgr A*. We suggest that a significant or even dominant fraction of this signal may be produced by several thousand late-type main-sequence stars that possibly hide in the central ~0.1 pc region of the Galaxy. As a result of tidal spin-ups caused by close encounters with other stars and stellar remnants, these stars should be rapidly rotating and hence have hot coronae, emitting copious amounts of X-ray emission with temperatures kT<~ a few keV. The Chandra data thus place an interesting upper limit on the space density of (currently unobservable) low-mass main-sequence stars near Sgr A*. This bound is close to and consistent with current constraints on the central stellar cusp provided by infrared observations. If coronally active stars do provide a significant fraction of the X-ray luminosity of Sgr A*, it should be variable on hourly and daily time scales due to giant flares occurring on different stars. Another consequence is that the quiescent X-ray luminosity and accretion rate of the SMBH are yet lower than believed before.

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